1. 1 A.Zalewska, Epiphany 2006 Introduction Agnieszka Zalewska Epiphany Conference on Neutrinos and Dark Matter, 6.01.2006 2006 Epiphany Conference on Neutrinos and Dark Matter as compared to 2000 Epiphany Conference on Neutrinos in Physics and Astrophysics

2. 2 A.Zalewska, Epiphany 2006 Neutrino sources from hep-ex/0211035 Experiments study solar, reactor, atmospheric, accelerator and UHE astrophysical neutrinos

3. 3 A.Zalewska, Epiphany 2006 At the time of Epiphany 2000  The main conference highlight was the evidence for oscillations of atmospheric neutrinos in SuperKamiokande  „Solar puzzle” was not yet resolved: SNO was at startup of data taking  Accelerator experiments: K2K had collected data for less than one year, Minos and MiniBOONE were under construction, CNGS experiments were before a formal approval  Reactor experiments: CHOOZ analysis was well advanced, KamLAND was under construction  Astrophysical HE neutrinos: experiments under construction  Many interesting theoretical ideas

4. 4 A.Zalewska, Epiphany 2006 Between 2000 and 2006  Solid experimental evidence for neutrino oscillations coming from the SuperKamiokande, K2K, SNO and KamLAND experiments (J.Zalipska on K2K) SuperKamiokande KamLAND SNO 1 ktona D 2 O 1 ktona, scyntylatora 50 kton H 2 O

5. 5 A.Zalewska, Epiphany 2006 Rate + Shape: Oscillations at 99.999995% C.L.  KamLAND: Testing the Model with L/E Behavior KamLAND, PRL 94, 2005 J.Klein, EPS HEP2005

6. 6 A.Zalewska, Epiphany 2006 Three neutrino mixing Atmospheric neutrinos CP phase solar neutrinos connects solar and atmospheric regions Oscillation parameters: 3 mixing angles, 2 differences of mass squared, 1 phase If neutrino is a Majorana particle, 2 additional phases If  then CP is violated for leptons (like for quarks),  13 is very important for a measurement of 

7. 7 A.Zalewska, Epiphany 2006 Oscillation parameters The most probable values:  23 = 45 0 (maximal mixing),  12 = 33 0 (large),  13 < 10 0 (small),  m 2 23  2.5 x 10 -3 eV 2,  m 2 12  8 x 10 -5 eV 2, |  m 2 13 |=|  m 2 23 -  m 2 12 | Why this scheme of mixing angles is so much different from the scheme for quark mixing?

8. 8 A.Zalewska, Epiphany 2006 Between 2000 and 2006  MINOS started data taking at the beginning of 2005 (first results from the beam are discussed these days at the collaboration meeting in Oxford) (D. Kiełczewska)  MiniBOONE has been running since 2002 - first results should be presented during the first half of 2006  OPERA will start data taking in 2006 (R. Zimmermann)  Big LAr detector „a la Icarus” should be redesigned

9. 9 A.Zalewska, Epiphany 2006 Three oscillation regions Two oscillation regions with a very solid experimental evidence: atmospheric region solar region Third region: LSND being checked by the MiniBOONE experiment If confirmed, a 4 th neutrino is required

10. 10 A.Zalewska, Epiphany 2006 LSND effect Excess of positrons above background interpreted as anty- e appearance due to oscillations

11. 11 A.Zalewska, Epiphany 2006  MiniBooNE – checking the LSND effect Results expected ~end of 2005 è 8 GeV protons from the Fermilab booster neutrino beam of energy about 1 GeV è detector at a distance of 500 m from the target è 10 21 p.o.t. to confirm/exclude the LSND effect

12. 12 A.Zalewska, Epiphany 2006 If MiniBOONE confirms LSND... revolution ! = 2.5 x 10 -3 eV 2 = 8 x 10 -5 eV 2

13. 13 A.Zalewska, Epiphany 2006 T3000 – by cloning 300t modules – canceled in 2005 40m The ICARUS experiment 20 m 4 th December 2004 Existing T600 detector – 600t of LAr T600 detector – installation in Gran Sasso Bigger monolithic detector – worshop in March 2006

14. 14 A.Zalewska, Epiphany 2006 T600 – data quality – from 2001 tests Hadronic interaction Muon bundle Richness of a single event     e 1 (9 MeV ) e + e - pair (24 MeV ) (2.5 MeV ) Collection view EM shower „Electronic bubble chamber” 7 publications based on this data

15. 15 A.Zalewska, Epiphany 2006 ICARUS experiment Responsibility of the Polish groups: production of anode wires (about 55000 in total) for TPC chambers of the future modules Original plan for the detector upgrade: four modules, each of 300 tons of LAr, to be constructed in the years 2005-2007 4 th December 2004

16. 16 A.Zalewska, Epiphany 2006 At the time of Epiphany 2006  Neutrino oscillations: Oscillation experiments enter a period of precise measurements – intense sources of neutrinos and huge detectors are needed as well as good theoretical tools to answer the following questions: Is  23 really maximal? How small is  13 ? Mass hierarchy – normal or inverted? Is CP violated for neutrinos? - talks by D.Kiełczewska, D.Motta, K.Long, A.Blondel, S.Katsanevas, J.Sobczyk, M.Rolinec

17. 17 A.Zalewska, Epiphany 2006 High intensity sources of neutrinos New type of accelerator: neutrinos from decays of accelerated muons (K.Long, A.Blondel) New type of accelerator: neutrinos (antineutrinos) from accelerated 18 Ne ( 6 He) (S.Katsanevas)  beams recent idea Conventional beams of v. high intensity (D.Kiełczewska)

18. 18 A.Zalewska, Epiphany 2006 Neutrino mass hierarchy Two important questions: Normal hierarchy (above) or inverted hierarchy (w.r.t.  m 2 atm ) How far from zero the whole picture is?

19. 19 A.Zalewska, Epiphany 2006 At the time of Epiphany 2006  Neutrino mass: Direct measurement based on the electron spectrum from the Tritium  decay in the KATRIN experiment (J.Bonn)

20. 20 A.Zalewska, Epiphany 2006 At the time of Epiphany 2006  Is neutrino a Majorana or a Dirac particle? Searches for neutrinoless double beta decays – many experiments proposed – observation of such a decay would be a great discovery - talks by K.Zuber, M.Wójcik, A.Bobyk

21. 21 A.Zalewska, Epiphany 2006 Dark Energy 73% Neutrinos 0.1  2% 0.1  2% Dark Matter 23% Ordinary Matter 4% (of this only about 10% luminous) 10% luminous) At the time of Epiphany 2006  Dark Matter searches One should remember that only 15 years ago neutrinos were serious candidates for Dark Matter, nowadays WIMPs (Weakly Interacting Massive Particles) are in fashion - talks by Ch.Sander, B.Baret, M.Sapiński, A.Szelc  High level theory by B.F.L. Ward

22. 22 A.Zalewska, Epiphany 2006 At the time of Epiphany 2006  Increasing synergy between particle physics and astrophysics and intense discussions about the future initiatives in both fields Will be reflected by many talks but especially by S.Katsanevas, J.Engelen, Ch.Spiering and S.Pokorski